REVIEW 6 cited by
Dust in Proto-Planetary Disks: Properties and Evolution
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
We review the properties of dust in protoplanetary disks around optically visible pre-main sequence stars obtained with a variety of observational techniques, from measurements of scattered light at visual and infrared wavelengths to mid-infrared spectroscopy and millimeter interferometry. A general result is that grains in disks are on average much larger than in the diffuse interstellar medium (ISM). In many disks, there is evidence that a large mass of dust is in grains with millimeter and centimeter sizes, more similar to "sand and pebbles" than to grains. Smaller grains (with micron-sizes) exist closer to the disk surface, which also contains much smaller particles, e.g., polycyclic aromatic hydrocarbons. There is some evidence of a vertical stratification, with smaller grains closer to the surface. Another difference with ISM is the higher fraction of crystalline relative to amorphous silicates found in disk surfaces. There is a large scatter in dust properties among different sources, but no evidence of correlation with the stellar properties, for samples that include objects from intermediate to solar mass stars and brown dwarfs. There is also no apparent correlation with the age of the central object, over a range roughly between 1 and 10 Myr. This suggests a scenario where significant grain processing may occur very early in the disk evolution, possibly when it is accreting matter from the parental molecular core. Further evolution may occur, but not necessarily rapidly, since we have evidence that large amounts of grains, from micron to centimeter size, can survive for periods as long as 10 Myr.
Forward citations
Cited by 6 Pith papers
-
Chemical Divergence and Water Depletion: Gas Properties of Evolved Upper Scorpius Disks Revealed by JWST/MIRI
JWST/MIRI survey of 2-6 Myr Upper Scorpius disks finds diverse chemotypes, 10-1000x lower water luminosities, and evidence that outer dust traps control inner-disk chemistry.
-
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): I. Program Overview and Summary of First Results
First systematic ALMA survey of protoplanetary gas finds median gas disk mass declining from about 6 Jupiter masses in under 1 Myr disks to about 0.5 Jupiter masses by 2 to 6 Myr, with a non-monotonic gas-to-dust rati...
-
Spatial distribution of water ice in the protoplanetary silhouette disk d216-0939
A radiative transfer model of the edge-on disk d216-0939 indicates 5.4% crystalline water ice in the cold outer layers, implying outward transport of ice.
-
Gravitational Sedimentation and Rebound of Strongly Coupled Dusty Plasma Crystals: A Molecular Dynamics Study
Molecular-dynamics simulations show that falling Yukawa-coupled dust crystals preserve hexagonal order, rebound layer-by-layer from a wall, and gradually degrade ABA stacking without losing collective motion.
-
Pristine composition or size evolution: Can current dust models reproduce emissivities observed in nearby protostars?
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
-
An Introduction to Dust Evolution and Vertical Transport in Protoplanetary Disks
A tutorial that reviews the physics and observational methods for measuring dust sizes and vertical settling in protoplanetary disks.
Discussion (0). Sign in to comment.